Dilution of chemical enrichment in galaxies 600 Myr after the Big Bang

Heintz, K. E.; Brammer, Gabriel; Giménez-Arteaga, Clara; Lagos, Claudia del P.; Vijayan, Aswin P.; Matthee, Jorryt; Watson, Derrick G.; Mason, Charlotte; Hutter, Anne; Toft, Sune; Fynbo, J. P. U.; Oesch, Pascal; Strait, Victoria B.

doi:10.48550/arxiv.2212.02890

Cited by 10 publications

(27 citation statements)

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“…Comparing this metallicity to other strong-line diagnostics defined for local "analogs" of high-redshift galaxies (Bian et al 2018) yields offsets of −0.2, 0.4, and −0.3 dex for the R23, O32, and O3Hβ calibrations, respectively. The most accurate calibration for this particular galaxy seems to be the O32 calibration from the Sloan Digital Sky Survey reference sample in Bian et al (2018), similar to the O32 diagnostics derived by Curti et al (2020), which seems to be consistent with the direct metallicity within 0.1 dex (as is also evident from the galaxy at z = 9.5 presented by Heintz et al 2022b).…”

Section: Rest-frame Nebular Line Emission and Metallicitysupporting

confidence: 72%

“…Our SFR and M å measurements for instance predict 12 log + (O/H) = 7.76, about 0.6 dex higher than that derived from the strong-line diagnostics. This offset appears to be ubiquitous in high-z galaxies at z  5 (Heintz et al 2022b), likely indicating substantial infall of neutral, pristine gas diluting the metallicity at z  5. Intriguingly, S04590 shows a pair of mass and metallicity measurements similar to those of the local, extremely metal-poor galaxy I Zwicky 18 (I Zw 18), which is characterized by an oxygen abundance of .…”

Section: Rest-frame Nebular Line Emission and Metallicitymentioning

confidence: 95%

“…Chemical abundances have also been derived for foreground galaxies toward background sources such as gamma-ray bursts and quasars out to z  6 (Hartoog et al 2015;Simcoe et al 2020;Saccardi et al 2022), which, however, only represent a single line of sight through the absorbing galaxies. Now with the advent of JWST we are able to derive robust, total gas-phase metallicities through the strong-line diagnostics of the most prominent nebular emission lines of galaxies during the first Gyr of cosmic time (e.g., Curti et al 2023;Heintz et al 2022b;Rhoads et al 2023;Schaerer et al 2022;Tacchella et al 2022). Crucially, these observations have also revealed prominent detections of the auroral [O III] λ4363 emission line, which enables direct T e -based metallicity measurements, which is necessary to consider since the typical strong-line diagnostics have only been calibrated to local z ≈ 0 galaxy samples.…”

Section: Introductionmentioning

confidence: 99%

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The Gas and Stellar Content of a Metal-poor Galaxy at z = 8.496 as Revealed by JWST and ALMA

Heintz

Giménez-Arteaga

Fujimoto

et al. 2023

ApJL

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We present a joint analysis of the galaxy S04590 at z = 8.496 based on NIRSpec, NIRCam, and NIRISS observations obtained as part of the Early Release Observations program of the James Webb Space Telescope (JWST) and the far-infrared [C ii] 158 μm emission line detected by dedicated Atacama Large Millimeter/submillimeter Array (ALMA) observations. We determine the physical properties of S04590 from modeling of the spectral energy distribution (SED) and through the redshifted optical nebular emission lines detected with JWST/NIRSpec. The best-fit SED model reveals a low-mass (M ⋆ = 107.2–108 M ⊙) galaxy with a low oxygen abundance of 12 + log ( O / H ) = 7.16 − 0.12 + 0.10 derived from the strong nebular and auroral emission lines. Assuming that [C ii] effectively traces the interstellar medium, we estimate the total gas mass of the galaxy to be M gas = (8.0 ± 4.0) × 108 M ⊙ based on the luminosity and spatial extent of [C ii]. This yields an exceptionally high gas fraction, f gas = M gas/(M gas + M ⋆) ≳ 90%, though one still consistent with the range expected for low metallicity. We further derive the metal mass of the galaxy based on the gas mass and gas-phase metallicity, which we find to be consistent with the expected metal production from Type II supernovae. Finally, we make the first constraints on the dust-to-gas (DTG) and dust-to-metal (DTM) ratios of galaxies in the epoch of reionization at z ≳ 6, showing overall low mass ratios of logDTG < −3.8 and logDTM < −0.5, though they are consistent with established scaling relations and in particular with those of the local metal-poor galaxy I Zwicky 18. Our analysis highlights the synergy between ALMA and JWST in characterizing the gas, metal, and stellar content of the first generation of galaxies.

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Section: Rest-frame Nebular Line Emission and Metallicitysupporting

confidence: 72%

Section: Rest-frame Nebular Line Emission and Metallicitymentioning

confidence: 95%

Section: Introductionmentioning

confidence: 99%

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The Gas and Stellar Content of a Metal-poor Galaxy at z = 8.496 as Revealed by JWST and ALMA

Heintz

Giménez-Arteaga

Fujimoto

et al. 2023

ApJL

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“…Based on these calibrations, we find that the galaxies at z = 8 − 9 fall below the mass metallicity relations at z = 0 − 3 (e.g., Sanders et al 2021) extrapolated down to M star ∼ 10 7 M . This is generally consistent with the model predictions (e.g., Schaye et al 2015;Ma et al 2016;Pallottini et al 2022;Ucci et al 2023) and the recent JWST results of the mass-metallicity measurements at z = 5 − 9.5 (Matthee et al 2022a;Heintz et al 2022a), but with different calibrations (e.g., Bian et al 2018;Curti et al 2020). By applying the same R3 calibrations to these recent JWST results, we obtain 12 + log(O/H) 7.7 − 8.1 and 7.2 − 8.2 for the z = 5 − 7 field galaxies and the lensed galaxies at z = 7.5 − 9.5, respectively.…”

Section: Chemical Evolutionsupporting

confidence: 91%

“…Figure 5 presents the SFR-M star relation. For comparison, we show the main sequence estimated at z = 2 and z = 6 (Iyer et al 2018), recent JWST results for the sources spectroscopically confirmed at z = 7 − 13 (Tacchella et al 2022a;Williams et al 2022;Roberts-Borsani et al 2022;Heintz et al 2022a;Robertson et al 2022;Curtis-Lake et al 2022), recent HST+IRAC results for bright galaxies at z phot ∼ 8 − 9 (Tacchella et al 2022b), and the 16-84th percentile of the distribution of simulated galaxies at z = 7 − 8 (Yung et al 2019b(Yung et al , 2022Behroozi et al 2019Behroozi et al , 2020Nelson et al 2019;Wilkins et al 2022b,a). Note that we use the SED-based SFR estimate (Section 3.5), instead of using the Hβ line.…”

Section: Sfr Vs Mstarmentioning

confidence: 93%

CEERS Spectroscopic Confirmation of NIRCam-Selected z > 8 Galaxy Candidates with JWST/NIRSpec: Initial Characterization of their Properties

Fujimoto¹,

Haro²,

Dickinson³

et al. 2023

Preprint

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We present JWST NIRSpec spectroscopy for 11 galaxy candidates with photometric redshifts of z 9−13 and M UV ∈ [−21, −18] newly identified in NIRCam images in the Cosmic Evolution Early Release Science (CEERS) Survey. We confirm emission line redshifts for 7 galaxies at z = 7.762-8.998 using spectra at ∼ 1-5µm either with the NIRSpec prism or its three medium resolution (R ∼ 1000) gratings. For z 9 photometric candidates, we achieve a high confirmation rate of 90%, which validates the classical dropout selection from NIRCam photometry. No robust emission lines are identified in three galaxy candidates at z > 10, where the strong [Oiii] and Hβ lines would be redshifted beyond the wavelength range observed by NIRSpec, and the Lyman-α continuum break is not detected with the sensitivity of the current data. Compared with HST-selected bright galaxies (M UV −22) that are similarly spectroscopically confirmed at z 8, these NIRCam-selected galaxies are characterized by lower star formation rates (SFR 4 M yr −1 ) and lower stellar masses ( 10 8 M ), but with higher specific SFR ( 40 Gyr −1 ), higher [O iii]+Hβ equivalent widths ( 1100 Å), and elevated production efficiency of ionizing photons (log(ξ ion /Hz erg −1 ) 25.8) induced by young stellar populations (< 10 Myrs) accounting for 20% of the galaxy mass, highlighting the key contribution of faint galaxies to cosmic reionization. Taking advantage of the homogeneous selection and sensitivity, we also investigate metallicity and ISM conditions with empirical calibrations using the [O iii] 5008 /Hβ ratio. We find that galaxies at z ∼ 8 − 9 have higher SFRs and lower metallicities than galaxies at similar stellar masses at z ∼ 2 − 6, which is generally consistent with the current galaxy formation and evolution models.

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GN-z11: Witnessing the formation of second-generation stars and an accreting massive black hole in a massive star cluster

D’Antona,

Vesperini,

Calura

et al. 2023

A&A

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We explore the possibility of the N-rich young proto-galaxy GN-z11, recently observed at z = 10.6 by JWST, being the result of the formation of second generation stars from pristine gas and asymptotic giant branch (AGB) ejecta in a massive globular cluster or nuclear star cluster. We show that a second generation forming out of gas polluted by the ejecta of massive AGB stars and mixed with gas of a standard composition accounts for the unusually large N/O in the GN-z11 spectrum. The timing of the evolution of massive (4–7.5 M⊙) AGBs also provides a favorable environment for the growth of a central stellar mass black hole to the AGN stage observed in GN-z11. According to our model, the progenitor system was born when the age of the Universe was ≃260 − 380 Myr, well within the bounds of the pre-reionization epoch.

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Dilution of chemical enrichment in galaxies 600 Myr after the Big Bang

Cited by 10 publications

References 0 publications

The Gas and Stellar Content of a Metal-poor Galaxy at z = 8.496 as Revealed by JWST and ALMA

The Gas and Stellar Content of a Metal-poor Galaxy at z = 8.496 as Revealed by JWST and ALMA

CEERS Spectroscopic Confirmation of NIRCam-Selected z > 8 Galaxy Candidates with JWST/NIRSpec: Initial Characterization of their Properties

GN-z11: Witnessing the formation of second-generation stars and an accreting massive black hole in a massive star cluster

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